DOCSLIB.ORG

From Massive Stars to Supernovae

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
From Massive Stars to Supernovae ISSN 1783-3426 THE MASSIVE STAR NEWSLETTER formerly known as the hot star newsletter * No. 151 2016 January-February Editors: Philippe Eenens (University of Guanajuato) [email protected] Raphael Hirschi (Keele University) http://www.astroscu.unam.mx/massive_stars CONTENTS OF THIS NEWSLETTER: News Obituaries Paul Kunasz and David Hummer Fizeau exchange visitors program Abstracts of 18 accepted papers Classical Oe Stars in the Field of the Small Magellanic Cloud An Apparent Precessing Helical Outflow from a Massive Evolved Star: Evidence for Binary Interaction A Comprehensive Comparative Test of Seven Widely-Used Spectral Synthesis Models Against Multi- Band Photometry of Young Massive Star Clusters Modeling X-ray emission line profiles from massive star winds – A review Long-Wavelength, Free-Free Spectral Energy Distributions from Porous Stellar Winds The Runaways and Isolated O-Type Star Spectroscopic Survey of the SMC (RIOTS4) Eta Carinae's Thermal X-ray Tail Measured with XMM-Newton and NuSTAR Stellar modelling of Spica, a high-mass spectroscopic binary with a beta Cep variable primary component Observational signatures of past mass-exchange episodes in massive binaries: The case of HD149404 The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems Probing the Dragonfish star-forming complex: the ionizing population of the young massive cluster Mercer 30 Short-term variability and mass loss in Be stars I. BRITE satellite photometry of eta and mu Centauri Luminous blue variables: An imaging perspective on their binarity and near environment OB stars at the lowest Local Group metallicity. GTC-OSIRIS observations of Sextans A Herschel observations of the nebula M1-67 around the Wolf-Rayet star WR 124 The Massive Stellar Population of W49: A Spectroscopic Survey Line-driven ablation of circumstellar disks: I. Optically thin decretion disks of classical Oe/Be stars Analysis of the WN star WR 102c, its WR nebula, and the associated cluster of massive stars in the Sickle Nebula Jobs Two Faculty Positions in Astrophysics at Instituto de Astrofisica de Atacama, Copiapo (Chile) 11 postdoc positions at Instituto de Astrofisica de Canarias Postdoctoral position on Gaia and massive stars Meetings Bridging the gap: from massive stars to supernovae Frontiers of massive-star evolution and core-collapse supernovae Supernova Remnants: An Odyssey In Space After Stellar Death Potsdam Astrophysical Summer School "Quantitative Spectroscopy in Astrophysics" News Obituaries Paul Kunasz and David Hummer Dear colleagues, some of you might already have heard the sad news that David Hummer has passed away recently. I was just informed that also Paul Kunasz has died, already in August 2015. Together with Dimitri Mihalas, we thus lost, during the last year, three of the world-leading pioneers and experts on radiative transfer, stellar atmospheres and may more topics. As an example, you might remember the most influential series of papers on comoving frame transfer, published by Mihalas, Kunasz & Hummer in the 1970ies. I am sure that everybody will miss them. An obituary for Paul Kunasz can be found on http://www.legacy.com/obituaries/dailycamera/obituary.aspx?pid=175559352 and an obituary for David Hummer on http://www.dailycamera.com/features/ci_29348396/friends-peers-raise-final-pint-david-hummer-co Those of you who are not aware of David's other 'profession', as a founder of one of the first micro- breweries in the USA, might be particularly interested in the latter article. Jo Puls Weblink: Email: [email protected] Back to contents Fizeau exchange visitors program: call for applications (Now closed) J. Hron & L. Misoni European Interferometry Initiative The Fizeau exchange visitors program in optical interferometry funds (travel and accommodation) visits of researchers to an institute of his/her choice (within the European Community) to perform collaborative work and training on one of the active topics of the European Interferometry Initiative. The visits will typically last for one month, and strengthen the network of astronomers engaged in technical, scientific and training work on optical/infrared interferometry. The program is open for all levels of astronomers (Ph.D. students to tenured staff), non-EU based missions will only be funded if considered essential by the Fizeau Committee. Applicants are strongly encouraged to seek also partial support from their home or host institutions. The deadline for applications is March 15. Fellowships can be awarded for missions starting in May 2016. Further informations and application forms can be found at www.european-interferometry.eu The program is funded by OPTICON/FP7. Please distribute this message also to potentially interested colleagues outside of your community! Looking forward to your applications, Josef Hron & Laszlo Mosoni (for the European Interferometry Initiative) Reference: Deadline March 15 Status: Other Weblink: www.european-interferometry.eu Comments: Please circulate not later than March 1 Email: [email protected] Back to contents PAPERS Abstracts of 18 accepted papers Classical Oe Stars in the Field of the Small Magellanic Cloud Jesse B. Golden-Marx (1), M. S. Oey (1), J. B. Lamb (2), Andrew S. Graus (3), Aaron S. White (1) ((1) University of Michigan, (2) Nassau Community College, (3) University of California, Irvine) We present 29±1 classical Oe stars from RIOTS4, a spatially complete, spectroscopic survey of Small Magellanic Cloud (SMC) field OB stars. The two earliest are O6e stars, and four are earlier than any Milky Way (MW) Oe stars. We also find ten Ope stars, showing He~\textsc{i} infill and/or emission; five appear to be at least as hot as ∼O7.5e stars. The hottest, star 77616, shows He~\textsc{ii} disk emission, suggesting that even the hottest O stars can form decretion disks, and offers observational support for theoretical predictions that the hottest, fastest rotators can generate He+-ionizing atmospheres. Our data also demonstrate that Ope stars correspond to Oe stars earlier than O7.5e with strong disk emission. We find that in the SMC, Oe stars extend to earlier spectral types than in the MW, and our SMC Oe/O frequency, 0.26±0.04, is much greater than the MW value, 0.03±0.01. These results are consistent with angular momentum transport by stronger winds suppressing decretion disk formation at higher metallicity. In addition, our SMC field Oe star frequency is indistinguishable from that for clusters, which is consistent with the similarity between rotation rates in these environments, and contrary to the pattern for MW rotation rates. Thus, our findings strongly support the viscous decretion disk model and confirm that Oe stars are the high-mass extension of the Be phenomenon. Additionally, we find that Fe~\textsc{ii} emission occurs among Oe stars later than O7.5e with massive disks, and we revise a photometric criterion for identifying Oe stars to J−[3.6]≥0.1. Reference: Accepted for publication in ApJ Status: Manuscript has been accepted Weblink: http://arxiv.org/abs/1601.03405 Email: [email protected] Back to contents An Apparent Precessing Helical Outflow from a Massive Evolved Star: Evidence for Binary Interaction Ryan M. Lau$^{1,2}$, Matthew J. Hankins$^{1}$, Terry L. Herter$^{1}$, Mark R. Morris$^{3}$, Elisabeth A. C. Mills$^{4}$, Michael E. Ressler$^{2}$ 1 - Cornell Astronomy Department; 2 - Caltech/JPL; 3 - Department of Physics and Astronomy, UCLA; 4 - National Radio Astronomy Observatory Massive, evolved stars play a crucial role in the metal-enrichment, dust budget, and energetics of the interstellar medium; however, the details of their evolution are uncertain because of their rarity and short lifetimes before exploding as supernovae. Discrepancies between theoretical predictions from single-star evolutionary models and observations of massive stars have evoked a shifting paradigm that implicates the importance of binary interaction. We present mid- to far-infrared observations from the Stratospheric Observatory for Infrared Astronomy (SOFIA) of a conical ``helix'' of warm dust ($\sim180$ K) that appears to extend from the Wolf-Rayet star WR102c. Our interpretation of the helix is a precessing, collimated outflow that emerged from WR102c during a previous evolutionary phase as a rapidly rotating luminous blue variable. We attribute the precession of WR102c to gravitational interactions with an unseen compact binary companion whose orbital period can be constrained to $800\,\mathrm{d} < P < 1400$ d from the inferred precession period, $\tau_p \sim 1.4\times 10^4$ yr, and limits imposed on the stellar and orbital parameters of the system. Our results concur with the range of orbital periods ($P\lesssim 1500$ d) where spin-up via mass exchange is expected to occur for massive binary systems. Reference: arXiv:1512.07639 Status: Manuscript has been accepted Weblink: http://arxiv.org/abs/1512.07639 Comments: Revised version to be updated Tuesday 1/19/2016 Email: [email protected] Back to contents A Comprehensive Comparative Test of Seven Widely-Used Spectral Synthesis Models Against Multi-Band Photometry of Young Massive Star Clusters A. Wofford, S. Charlot, G. Bruzual, J. J. Eldridge, D. Calzetti, A. Adamo, M. Cignoni, S. E. de Mink, D. A. Gouliermis, K. Grasha, E. K. Grebel, J. Lee, G. Ostlin, L. J. Smith, L. Ubeda, E. Zackrisson Sorbonne Universites, UPMC-CNRS, UMR7095, Institut d’Astrophysique de Paris We test the predictions of spectral synthesis models based on seven different massive-star
Load more

Recommended publications
  • Mathématiques Et Espace
    Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée.
    [Show full text]
  • The Detection of 13CO and Other Apparent Abundance Anomalies In
    The Detection of 13CO and Other Apparent Abundance Anomalies in the Secondary Stars of Long-Period Cataclysmic Variables Thomas E. Harrison1,2, Heather L. Osborne2 Department of Astronomy New Mexico State University, Box 30001, MSC 4500, Las Cruces, NM 88003-8001 Steve B. Howell WIYN Observatory and National Optical Astronomy Observatories, 950 North Cherry Avenue, Tucson, AZ 85726 Accepted for publication in the Astronomical Journal on 18 February, 2004 1Visiting Astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. 2Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University arXiv:astro-ph/0402470v1 19 Feb 2004 of Hawaii under contract from the National Aeronautics and Space Administration. Subject headings: cataclysmic variablesstars: infrared spectrastars: individual (V442 Centauri, SY Cancri, RU Pegasi, CH Ursae Majoris, MU Centauri, TT Crateris, AC Cancri, EM Cygni, V426 Ophiuchi, SS Cygni, BV Puppis, AH Herculis) Received ; accepted –2– ABSTRACT We present moderate resolution (R ≥ 1,800) infrared K-band spectra of twelve long-period (Porb ≥ 6 hr) cataclysmic variables. We detect absorption lines from the photospheres of the secondary stars in every system, even though two of them were undergoing outbursts. We have attempted to assign spectral types to each of the secondary stars, and these classifications are generally consistent with previous determinations/estimates. We find evidence for abundance anomalies that include enhancements and/or deficits for all of the species commonly found in K-band spectra of G- and K-type dwarfs.
    [Show full text]
  • The Brightest Stars Seite 1 Von 9
    The Brightest Stars Seite 1 von 9 The Brightest Stars This is a list of the 300 brightest stars made using data from the Hipparcos catalogue. The stellar distances are only fairly accurate for stars well within 1000 light years. 1 2 3 4 5 6 7 8 9 10 11 12 13 No. Star Names Equatorial Galactic Spectral Vis Abs Prllx Err Dist Coordinates Coordinates Type Mag Mag ly RA Dec l° b° 1. Alpha Canis Majoris Sirius 06 45 -16.7 227.2 -8.9 A1V -1.44 1.45 379.21 1.58 9 2. Alpha Carinae Canopus 06 24 -52.7 261.2 -25.3 F0Ib -0.62 -5.53 10.43 0.53 310 3. Alpha Centauri Rigil Kentaurus 14 40 -60.8 315.8 -0.7 G2V+K1V -0.27 4.08 742.12 1.40 4 4. Alpha Boötis Arcturus 14 16 +19.2 15.2 +69.0 K2III -0.05 -0.31 88.85 0.74 37 5. Alpha Lyrae Vega 18 37 +38.8 67.5 +19.2 A0V 0.03 0.58 128.93 0.55 25 6. Alpha Aurigae Capella 05 17 +46.0 162.6 +4.6 G5III+G0III 0.08 -0.48 77.29 0.89 42 7. Beta Orionis Rigel 05 15 -8.2 209.3 -25.1 B8Ia 0.18 -6.69 4.22 0.81 770 8. Alpha Canis Minoris Procyon 07 39 +5.2 213.7 +13.0 F5IV-V 0.40 2.68 285.93 0.88 11 9. Alpha Eridani Achernar 01 38 -57.2 290.7 -58.8 B3V 0.45 -2.77 22.68 0.57 144 10.
    [Show full text]
  • Be Stars Seen by Space Photometry
    Be Stars Seen by Space Photometry Thomas Rivinius1, Dietrich Baade2 and Alex C. Carciofi3 1. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile 2. ESO | European Organisation for Astronomical Research in the Southern Hemisphere, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 3. Instituto de Astronomia, Geof´ısica e Ci^encias Atmosf´ericas, Universidade de S~ao Paulo, 05508-900, S~ao Paulo, SP, Brazil Classical Be stars are introduced as object class and their particular potential for space based photometry is highlighted. A brief summary of the various types of variability observed in Be stars makes clear that an interpretation of every single frequency as a pulsation mode falls short, instead there are as well purely circumstellar variations and those that originate in the immediate stellar to cir- cumstellar interaction region. In particular the latter offer great potential, as they are linked to one of the few remaining great riddles of Be stars, namely how they feed their disks. 1 Introduction The class of Be stars is simply defined as those non-supergiant B stars that at least once have shown Balmer line emission (see Rivinius et al., 2013, for a review). While this definition is very valuable for bulk classification of stars for which no high quality data is available, e.g., in the Magellanic Clouds, it is also very broad: Any circumstellar gas close to a B star and above some threshold density will produce line emission. In an attempt at a taxonomy that reflects our knowledge on how the gas was put and is kept close to the star (e.g., magnetically confined, an accretion disk, or a decretion disk), the class was subdivided.
    [Show full text]
  • Newsletter 138 of Working Group on Massive Star
    ISSN 1783-3426 THE MASSIVE STAR NEWSLETTER formerly known as the hot star newsletter * No. 138 2013 November-December Editors: Philippe Eenens (University of Guanajuato) [email protected] Raphael Hirschi (Keele University) http://www.astroscu.unam.mx/massive_stars CONTENTS OF THIS NEWSLETTER: News Obituary Dimitri Mihalas VLTI Observatory survey at High Angular resolution of Active OB stars Abstracts of 18 accepted papers The IACOB project: I. Rotational velocities in Northern Galactic O and early B-type stars revisited. The impact of other sources of line-broadening HI Lyman-alpha equivalent widths of stellar populations Modeling Tracers of Young Stellar Population Age in Star-Forming Galaxies The Dynamics of Ultracompact HII Regions Optical spectra of 5 new Be/X-ray Binaries in the Small Magellanic Cloud and the link of the supergiant B[e] star LHA 115-S 18 with an X-ray source On the origin of variable structures in the winds of hot luminous stars Wind collisions in three massive stars of Cyg OB2 Discovery of the first B[e] supergiants in M 31 Constraints on Massive Star Formation: Cygnus OB2 was always an Association The feedback of massive stars on interstellar astrochemical processes The VLT-FLAMES Tarantula Survey. XIII: On the nature of O Vz stars in 30 Doradus The eccentric massive binary V380 Cyg: revised orbital elements and interpretation of the intrinsic variability of the primary component The incidence of stellar mergers and mass gainers among massive stars The surface nitrogen abundance of a massive star in relation to its oscillations, rotation, and magnetic field The Galactic O-Star Spectroscopic Survey (GOSSS).
    [Show full text]
  • COMMISSION 27 of the I.A.U. INFORMATION BULLETIN on VARIABLE STARS Nos. 3001
    COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Nos. 3001 - 3100 1987 March - 1987 October EDITORS: L. SZABADOS and B. SZEIDL KONKOLY OBSERVATORY H-1525 BUDAPEST P.O. Box 67, HUNGARY HU ISSN 0374 - 0676 CONTENTS 3001 PHOTOELECTRIC ELEMENTS AND REVISED SPECTRAL TYPES OF XX Cas R.K. Srivastava 18 March 1987 3002 HR 2554 - A POSSIBLE NEW Zeta Aur SYSTEM Thomas B. Ake, S.B. Parsons 19 March 1987 3003 53 PISCIUM - LARGER AMPLITUDE Marek Wolf 23 March 1987 3004 OBSERVATIONS AND A TIME OF MINIMUM OF TV Cet Daniel B. Caton, R. Lee Hawkins 25 March 1987 3005 ON THE PRIMARY MINIMUM OF ECLIPSING BINARY AY Cam J.B. Srivastava, C.D. Kandpal 30 March 1987 3006 AN UNEXPECTEDLY EARLY FADING OF V644 Cen (CPD -60d3278) J.K. Davies, A. Evans, M.F. Bode, D.C.B Whittet 3 April 1987 3007 PHOTOELECTRIC OBSERVATIONS OF TT ARIETIS ON 1/2 OCTOBER 1986 S. Rossiger 6 April 1987 3008 DELTA Cap: A POSSIBLE RS CVn BINARY R.K. Srivastava 9 April 1987 3009 ON THE CONSTANCY OF SOME STARS IN NGC 2287 = MESSIER 41 Brian A. Skiff 13 April 1987 3010 AN IMPROVEMENT OF THE ROTATIONAL PERIOD OF CQ UMa Zdenek Mikulasek 16 April 1987 3011 CORRECT PERIOD OF THE ECLIPSING STAR MN AURIGAE H. Gessner 16 April 1987 3012 JHK LIGHT CURVES OF CG CYGNI J.K. Davies, D.K. Bedford, J.J. Fuensalida, M.J. Arevalo 17 April 1987 3013 OPTICAL BEHAVIOUR OF THE X-RAY BINARY V1727 CYGNI = 4U 2129+47 IN 1986 W.
    [Show full text]
  • Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1
    Effects of Rotation Arund the Axis on the Stars, Galaxy and Rotation of Universe* Weitter Duckss1 1Independent Researcher, Zadar, Croatia *Project: https://www.svemir-ipaksevrti.com/Universe-and-rotation.html; (https://www.svemir-ipaksevrti.com/) Abstract: The article analyzes the blueshift of the objects, through realized measurements of galaxies, mergers and collisions of galaxies and clusters of galaxies and measurements of different galactic speeds, where the closer galaxies move faster than the significantly more distant ones. The clusters of galaxies are analyzed through their non-zero value rotations and gravitational connection of objects inside a cluster, supercluster or a group of galaxies. The constant growth of objects and systems is visible through the constant influx of space material to Earth and other objects inside our system, through percussive craters, scattered around the system, collisions and mergers of objects, galaxies and clusters of galaxies. Atom and its formation, joining into pairs, growth and disintegration are analyzed through atoms of the same values of structure, different aggregate states and contiguous atoms of different aggregate states. The disintegration of complex atoms is followed with the temperature increase above the boiling point of atoms and compounds. The effects of rotation around an axis are analyzed from the small objects through stars, galaxies, superclusters and to the rotation of Universe. The objects' speeds of rotation and their effects are analyzed through the formation and appearance of a system (the formation of orbits, the asteroid belt, gas disk, the appearance of galaxies), its influence on temperature, surface gravity, the force of a magnetic field, the size of a radius.
    [Show full text]
  • Talks Antofagasta, March 1-4, 2016 1
    XIII Annual Meeting of the Chilean Astronomical Society Book of abstracts - Talks Antofagasta, March 1-4, 2016 1 Claudia Agliozzo Universidad Nacional Andrés Bello A tale of the mass-loss of the magellanic LBV R127 During their lifetime, Luminous Blue Variable stars (LBVs) must rapidlyexpel their H envelope, with the highest mass-loss rates (> 10^(-5) M_sun/yr), in order to evolve into Wolf-Rayet stars.However, the physical mechanism underlying the mass-loss is not yet understood.I present our extraordinary multi- wavelength dataset of R127, a famousLBV in the Large Magellanic Cloud, widely observed in the past at visiblewavelengths. Our dataset comprises high-resolution centimetre ATCA and submillimetre ALMA data, in addition to new high-spectral resolution optical data acquired with the instrument MIKE at Magellan II telescope.As shown by the different spectral features detected, the mass-loss ishighly complex, with signatures of different episodes, such as have beenseen in previous spectroscopic observations and in the galactic prototypeLBV AG Carinae. We newly discover that from theinner to the outer regions, the stellar wind changes geometry.With all our data together, the picture seems much clearer: theasymmetric morphology of the wind and of the circumstellar nebula aremore likely due to external factors than intrinsic asymmetriesof the mass-loss. I will discuss different scenarios.We don't know yet how common this behaviour is in galactic and magellanic LBVs. However, noticeably, the geometry of the nebula resembles that of Eta Carinae and of the blue-supergiant progenitor of Supernova 1987A. 2 Gustavo Aguayo Universidad de Concepción Optical study of the Be star Mu Centauri We present an optical study of the Be star Mu Centauri, this study was developed using spectroscopic data taken with CHIRON and CORALIE spectrograph, there were measured important parameters of some lines located at the optical range as equivalent width and peak separation, also correlations between equivalent widths of some lines were found and are presented here.
    [Show full text]
  • Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities
    Ground Based, Space Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Space Based, Technological Development, and State of the Profession Activities Ground Based, Space Based, and Technological Development Activities Ground Based and Space Based Activities Ground Based, Infrastructure, Technological Development, and State of the Profession Activities Ground Based, Infrastructure, Technological Development, State of the Profession, and Other Activities Ground Based, Infrastructure, and Technological Development Activities Ground Based, Infrastructure, and State of the Profession Activities Ground Based and Infrastructure Activities Ground Based, Technological Development, and State of the Profession Activities Ground Based and Technological Development Activities Ground Based Projects Space Based, Infrastructure, Technological Development, and State of the Profession Activities Space Based, Infrastructure, Technological Development Activities Space Based and Infrastructure Activities Space Based, Technological Development, and State of the Profession Activities Space Based and Technological Development Activities Space Based and State of the Profession Activities Space Based Projects Infrastructure, Technological Development, and State of the Profession Activities Infrastructure, Technological Development, and Other Activities Infrastructure and Technological Development Activities Infrastructure, State of the Profession, and Other Activities Infrastructure and State of the Profession
    [Show full text]
  • Variable Star Section
    No. 21 (C1996) PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND A GENERAL INDEX by Stars, Subjects and Authors to Publications No. 1-20 Director: Frank M. Bateson P.O. Box 3093 Greerton, tauranga New Zealand ISSN 0111-736X PUBLICATIONS OF THE VARIABLE STAR SECTION ROYAL ASTRONOMICAL SOCIETY OF NEW ZEALAND No. 21 CONTENTS 1. A GENERAL INDEX TO THE PUBLICATIONS OF THE VARIABLE STAR SECTION (R.A.S.N.Z.) NUMBERS 1-20 G.W. Christie, Ranald Mcintosh and O.R. Hull 2. INDIVIDUAL STARS 15. SUBJECT INDEX 24. AUTHOR INDEX 1996 July 20th PubL Variable Star Section, RASNZ ©Astronomical Research Ltd 21:1-28 General Index to the Publications of the Variable Star Section (R.A.S.N.Z.) Numbers 1-20 G.w. CHRISTIE1, RANALD MCINTOSH2 AND O.R. HULL3 'Auckland Observatory, Auckland, New Zealand Electronic matt [email protected] 'Variable Star Section, RASNZ Electronic mail: [email protected] 'Variable Star Section, RASNZ Abstract: A cummulative index to the first twenty issues of the Publications of the Variable Star Section (R. A.S.N.Z.) covering the period 1973 to 1995 is presented. 1. EXPLANATION The following index is divided into three sections. The first part is the index to Individual Stars, the second part is the Subject Index and the third part is the Author Index. In all sections, each entry consists of the title of the paper followed by the list of authors, the Publication number in parentheses, the page number and finally the nominal year of publication, also in parentheses.
    [Show full text]
  • Newsletter 98 ª December 1999 NEWSLETTER
    Newsletter 98 ª December 1999 NEWSLETTER The American Astronomical Societys2000 Florida Avenue, NW, Suite 400sWashington, DC [email protected] AAS ELECTIONS PRESIDENT’S COLUMN ELECTION BALLOT, AMENDMENTS Bob Gehrz, President, [email protected] TO THE CONSTITUTION AND We did it! Thank you, members of the American CANDIDATE STATEMENTS Astronomical Society, for A large part of this issue is devoted to the AAS Election. The your vigorous participation enclosed ballot lists not only candidates who stand for election in our campaign to avert a to AAS Office, but includes an important vote on amendments funding disaster for the to the AAS Constitution proposed by the Council. astronomy and space Candidate statements begin on page 2. science communities. Our combination of letters, The discussion of the proposed amendments begins on page 4. phone calls, FAXes and • Please vote both sides of the ballot. one-on-one meetings • Vote for no more candidates than the number indicated for enabled us to dodge a each position. dangerous budget bullet. • Sign the envelope and use it to return your ballot to the In the final bill that resulted “More powerful than a locomotive, ...” Office of the Secretary by Monday, 31 January 2000. from the House/Senate Conference, NASA’s Gehrz rallied the AAS to stop the speeding • Safeguard your ballot; we cannot send a replacement should budget train before it derailed the US appropriation was higher it be lost. astronomy program. than either the Senate and House had initially proposed. NSF, overall, received more than 2nd CENTURY FUND GROWS! a 7% increase in its budget.
    [Show full text]
  • Dimitri Mihalas
    Dimitri Mihalas Dear colleagues of the massive star community, you might have heard already that Dimitri Mihalas has passed away last Thursday, after serious illness. This is very sad news for us all. According to Ivan Hubeny, just one day before his death Dimitri saw the more or less final manuscript of their new book on Stellar Atmospheres. This and all his other books, as well as our memories, will make him immortal to us. Please find enclosed the official obituary from Los Alamos. Obituary World-renowned astrophysicist Dimitri Mihalas passed away in his sleep at his home on November 21, 2013 in Santa Fe, New Mexico. Dr. Mihalas retired from the University of Illinois at Urbana-Champaign in 1999 and from the Los Alamos National Laboratory in 2011. Dimitri, to his friends and family, has donated his body to the University of New Mexico Medical School and his library to New Mexico Tech. Dimitri was born on March 20, 1939 in Los Angeles, California where he grew up. He received his B. A., with Highest Honors, in three majors: Physics, Mathematics, and Astronomy from the University of California at Los Angeles at age 20. Four years later he received his Ph. D in Astronomy and Physics from the California Institute of Technology. He then joined the faculty of the Department of Astrophysical Sciences at Princeton University. In the following three decades, he was a professor in the Department of Astronomy at the University of Chicago, the University of Colorado at Boulder, and the University of Illinois at Urbana-Champaign.
    [Show full text]